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To explore the magnetic flux dispersion in the undisturbed solar photosphere,magnetograms acquired by Helioseismic and Magnetic Imager (HMI) onboard theSolar Dynamic Observatory (SDO) were utilized. Two areas, a coronal hole area(CH) and an area of super-granulation pattern, SG, were analyzed. We exploredthe displacement and separation spectra and the behavior of the turbulentdiffusion coefficient, $K$. The displacement and separation spectra are verysimilar to each other. Small magnetic elements (of size 3-100 squared pixelsand the detection threshold of 20 Mx sm$^{-2}$) in both CH and SG areasdisperse in the same way and they are more mobile than the large elements (ofsize 20-400 squared pixels and the detection threshold of 130 Mx sm$^{-2}$).The regime of super-diffusivity is found for small elements ($\gamma \approx1.3 $ and $K$ growing from $\sim$100 to $\sim$ 300 km$^2$ s$^{-1}$). Largeelements in the CH area are scanty and show super-diffusion with $\gamma\approx 1.2$ and $K$ = (62-96) km$^2$ s$^{-1}$ on rather narrow range of500-2200 km. Large elements in the SG area demonstrate two ranges of linearityand two diffusivity regimes: sub-diffusivity on scales (900-2500) km with$\gamma=0.88$ and $K$ decreasing from $\sim$130 to $\sim$100 km$^2$ s$^{-1}$,and super-diffusivity on scales (2500-4800) km with $\gamma \approx 1.3$ and$K$ growing from $\sim$140 to $\sim$200 km$^2$ s$^{-1}$. Comparison of ourresults with the previously published shows that there is a tendency ofsaturation of the diffusion coefficient on large scales, i.e., the turbulentregime of super-diffusivity is gradually replaced by normal diffusion.

Dispersion of the solar magnetic flux in undisturbed photosphere as derived from SDO/HMI data